Inverse mass cascade in dark matter flow and effects on halo deformation, energy, size, and density profiles

TL;DR

This paper investigates how inverse mass cascade influences dark matter halo properties, revealing effects on halo deformation, energy, size, and density profiles, and proposing models consistent with N-body simulations.

Contribution

It introduces a novel analysis of mass cascade effects on halo structure, including a new density profile model and equations of state based on radial flow and surface energy.

Findings

Fast mass accretion leads to expanding halo cores.

Radial flow induces a scale radius and non-isothermal density profiles.

Halo size follows a lognormal distribution and exhibits Brownian motion behavior.

Abstract

Inverse mass cascade is a key feature of the intermediate statistically steady state for self-gravitating collisionless dark matter flow (SG-CFD). This paper focus on effects of mass cascade on halo energy, momentum, dispersion, size, and density. Halo with fast mass accretion has an expanding core. Mass cascade forms a new layer of mass that deforms the original halo and induces nonzero radial flow (outwards in core and inwards in outer regions). The inward/outward flow leads to an extra length scale (scale radius) that is not present in isothermal profile. Halo concentration c=3.5 can be derived for fast growing halos. For cusp-core controversy, a double-power-law density is proposed as a result of nonzero radial flow. The inner/outer density are controlled by halo deformation rate and halo growth, respectively. The slower deformation at center, the steeper density. For fast growing halos, radial flow at center is simply Hubble flow that leads to the existence of central core. Mass cascade leads to nonzero halo surface energy/tension and radial flow that enhances dispersion in outer region. An effective exponent of gravity $n_e$=-1.3 (not -1) is obtained due to halo surface energy. Halo size follows a geometric Brownian motion and lognormal distribution. Brownian motion of particles in evolving halos leads to Fokker-Planck equations for particle distribution that is dependent on the radial and osmotic flow. Complete solutions of particle distribution are presented based on a simple model of osmotic flow. The proposed model agrees with N-body simulation for various halo group sizes. With reference pressure/density defined at center, equation of state can be established for relative pressure/density. Pressure, density, and dispersion at halo center are presented. The core size $x_c$ is obtained where Hubble flow is dominant. Simple closures are proposed for self-consistent halo density.